Observations of the Lb variable NO Aur.

Details Observations of the Lb variable NO Aur. Observations of the Lb variable NO Aur.

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996baavs..89....5l&link_type=abstract

Br. Astron. Assoc., Var. Star Sect. Circ., No. 89, p. 5 - 6

Astronomy and Astrophysics

Astronomy

Pulsating Stars: Observations, Pulsating Stars: Periods

Scientific paper

NO Aur (=HR 1939, HD 37536, BD +31°1049, SAO 58322) was discovered to be variable by Eggen (1967) on the basis of 5 photoelectric observations made over about 80 days in 1965 - 66. The star is relatively massive and highly evolved. It may be a pulsating AGB star. NO Aur was added to the VSS programme in 1973 and observed to 1988, and again in 1995. There are only a relatively small number of observations. The raw observations are spread fairly evenly between m 6.2 and 7.0 but there is a definite suggestion of long term activity. The power spectrum of the raw data shows a strong period at -2500 days, and even after the personal bias of the observers has been removed assuming that the star is constant this variation persists. The personal biases and the mean light curve were recalculated using 500 day bins. The best fit period is 2520±40 days. The fit is not perfect but given that these are visual observations and the amplitude is only 0.30 mag, the scatter is not unreasonable.

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